J/A+A/677/A33 38 Kepler and K2 systems RVs (Bonomo+, 2023)
Cold Jupiters and improved masses in 38 Kepler and K2 small-planet systems from
3661 HARPS-N radial velocities. No excess of cold Jupiters in small-planet
systems.
Bonomo A.S., Dumusque X., Massa A., Mortier A., Bongiolatti R.,
Malavolta L., Sozzetti A., Buchhave L.A., Damasso M., Haywood R.D.,
Morbidelli A., Latham D.W., Molinari E., Pepe F., Poretti E., Udry S.,
Affer L., Boschin W., Charbonneau D., Cosentino R., Cretignier M.,
Ghedina A., Lega E., Lopez-Morales M., Margini M., Martinez Fiorenzano A.F.,
Mayor M., Micela G., Pedani M., Pinamonti M., Rice K., Sasselov D.,
Tronsgaard R., Vanderburg A.
<Astron. Astrophys. 677, A33 (2023)>
=2023A&A...677A..33B 2023A&A...677A..33B (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Exoplanets
Keywords: planetary systems - planets and satellites: detection -
planets and satellites: formation -
planets and satellites: fundamental parameters -
techniques: radial velocities - methods: statistical
Abstract:
The exoplanet population characterized by relatively short orbital
periods (P<100d) around solar-type stars is dominated
by super-Earths and sub-Neptunes. However, these planets are missing
in our Solar System and the reason behind this absence is still
unknown. Two theoretical scenarios invoke the role of Jupiter as the
possible culprit: Jupiter may have acted as a dynamical barrier to the
inward migration of sub-Neptunes from beyond the water iceline;
alternatively, Jupiter may have considerably reduced the inward flux
of material (pebbles) required to form super-Earths inside that
iceline. Both scenarios predict an anti-correlation between the
presence of small planets and that of cold Jupiters in exoplanetary
systems.
To test that prediction, we homogeneously analyzed the radial-velocity
measurements of 38 Kepler and K2 transiting small planet systems
gathered over nearly ten years with the HARPS-N spectrograph, as well
as publicly available radial velocities collected with other
facilities. We used Bayesian differential evolution Markov chain Monte
Carlo techniques, which in some cases were coupled with Gaussian
process regression to model non-stationary variations due to stellar
magnetic activity phenomena. We detected five cold Jupiters in three
systems: two in Kepler-68, two in Kepler-454, and a very eccentric one
in K2-312. We also found linear trends caused by bound companions in
Kepler-93, Kepler-454, and K2-12, with slopes that are still
compatible with a planetary mass for outer bodies in the Kepler-454
and K2-12 systems.
By using binomial statistics and accounting for the survey
completeness, we derived an occurrence rate of 9.3+7.7-2.9% for
cold Jupiters with 0.3-13MJup and 1-10AU, which is lower but still
compatible at 1.3σ with the value measured from radial-velocity
surveys for solar-type stars, regardless of the presence or absence of
small planets. The sample is not large enough to draw a firm
conclusion about the predicted anti-correlation between small planets
and cold Jupiters; nevertheless, we found no evidence of previous
claims of an excess of cold Jupiters in small planet systems.
As an important byproduct of our analyses, we homogeneously determined
the masses of 64 Kepler and K2 small planets, reaching a precision
better than 5, 7.5, and 10σ for 25, 13, and 8 planets,
respectively. Finally, we release the 3661 HARPS-N radial velocities
used in this work to the scientific community. These radial-velocity
measurements mainly benefit from an improved data reduction software
that corrects for subtle prior systematic effects.
Description:
Orbital and physical parameters and HARPS-N radial velocity and
activity indicators for 38 Kepler and K2 systems.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 212 38 Kepler and K2 systems in our sample
tablea1.dat 291 65 Orbital and physical parameters of the 65
transiting Kepler and K2 planets
refs.dat 66 40 References
table2.dat 149 3661 HARPS-N measurements of radial velocity and
activity indicators
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See also:
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
IV/34 : K2 Ecliptic Plane Input Catalog (EPIC) (Huber+, 2017)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- System Name of the system
13- 26 A14 ---- OName Other name
28 A1 --- Mult [ms] Multiplicity of transiting planets
30- 34 F5.3 Msun Ms Stellar mass
36- 40 F5.3 Msun e_Ms Error on stellar mass (lower value)
42- 46 F5.3 Msun E_Ms Error on stellar mass (uuper value)
48- 53 F6.4 Rsun Rs Stellar radius
55- 60 F6.4 Rsun e_Rs Error on stellar radius (lower value)
62- 67 F6.4 Rsun E_Rs Error on stellar radius (uuper value)
69- 72 I4 K Teff Effective temperature
74- 76 I3 K e_Teff Effective temperature error
78- 83 F6.3 Gyr Age Age
85- 89 F5.3 Gyr e_Age Error on age (lower value)
91- 95 F5.3 Gyr E_Age Error on age (uuper value)
97 A1 --- l_[Fe/H] Limit flag on [Fe/H]
98-102 F5.2 [-] [Fe/H] ?=- Metallicity
104-107 F4.2 [-] e_[Fe/H] ? Error on [Fe/H] (lower value)
109-112 F4.2 [-] E_[Fe/H] ? Error on [Fe/H] (uuper value)
114-116 I3 --- NRV Number of radial velocities from all surveys
118-120 I3 --- NRVHN Number of HARPS-N radial velocities
122 I1 --- NDat Number of radial-velocity datasets
124 I1 --- n_NDat [1]? Note on NDat (1)
126-129 I4 d Dur Total duration of the radial-velocity
time series
131-212 A82 --- Refs Literature references for both the stellar
parameters and the radial-velocity
measurements (2)
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Note (1): Note as follows:
2 = Two datasets were considered for the HARPS-N data, because the
replacement of the red side of the HARPS-N CCD in late September
2012 resulted in a different zero point for the RVs gathered
after that epoch.
Note (2): Note for this work reference:
The new system parameters Ms, Rs, and Age were derived with the
public EXOFASTv2 tool by fitting the stellar SED and using the
MIST evolutionary tracks. Gaussian priors were imposed on the
Teff and [Fe/H], as derived from the analysis of the HARPS-N
spectra, and on stellar parallax from Gaia EDR3 (see text for
more details).
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Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 12 A12 --- Name Planet name
13- 27 A15 --- OName Other planet name
29- 40 F12.7 d Tc Transit mid-time
42- 50 F9.7 d e_Tc Transit mid-time error
51- 63 F13.9 d Per Orbital period
65- 75 F11.9 d e_Per Orbital period error
77 I1 --- n_Per [2]? Note on Per (1)
79- 84 F6.4 Rgeo Rp Planetary radius
86- 91 F6.4 Rgeo e_Rp Planetary radius error (lower value)
93- 98 F6.4 Rgeo E_Rp Planetary radius error (upper value)
100-105 F6.3 deg i Orbital inclination
107-112 F6.3 deg e_i Orbital inclination error (lower value)
114-118 F5.3 deg E_i Orbital inclination error (upper value)
120-129 A10 --- Ref Refeferences for the transit parameters,
in refs.dat file (2)
131 A1 --- l_e Limit flag on e
132-136 F5.3 --- e Orbital eccentricity
138-142 F5.3 --- e_e ? Orbital eccentricity error
144 A1 --- n_e [f] f for fixed
146 A1 --- l_K Limit flag on K
147-150 F4.2 m/s K Radial-velocity semi-amplitude
152-155 F4.2 m/s e_K ? Radial-velocity semi-amplitude error
(lower value)
157-160 F4.2 m/s E_K ? Radial-velocity semi-amplitude error
(upper value)
162 A1 --- l_Mp Limit flag on Mp
163-167 F5.2 Mgeo Mp Planet mass
169-174 F6.3 Mgeo e_Mp ? Planet mass error (lower value)
176-180 F5.2 Mgeo E_Mp ? Planet mass error (upper value)
182 A1 --- l_rhop Limit flag on rhop
183-189 F7.3 g/cm3 rhop Density error
191-194 F4.2 g/cm3 e_rhop ? Density error (lower value)
196-199 F4.2 g/cm3 E_rhop ? Density error (upper value)
201 A1 --- l_loggp Limit flag on loggp
202-206 F5.3 [cm/s2] loggp Surface gravity
208-212 F5.3 [cm/s2] e_loggp ? Surface gravity error (lower value)
214-218 F5.3 [cm/s2] E_loggp ? Surface gravity error (upper value)
220-226 F7.5 AU a Semi-major axis
228-234 F7.5 AU e_a Semi-major axis error (lower value)
236-242 F7.5 AU E_a Semi-major axis error (upper value)
244-249 F6.1 K Teq Equilibrium temperature (3)
251-254 F4.1 K e_Teq Equilibrium temperature error
256-263 F8.3 Earth Fp Stellar incident flux (in Earth flux unit)
265-271 F7.3 Earth e_Fp Stellar incident flux error (lower value)
(in Earth flux unit)
273-279 F7.3 Earth E_Fp Stellar incident flux error (upper value)
(in Earth flux unit)
281-291 A11 --- System System name
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Note (1): Note as follows:
8 = The orbital period of K2-2b comes from the RVs by imposing a Gaussian
prior on Tc only, and slightly differs from the value reported in
Vanderburg et al. (2015ApJ...800...59V 2015ApJ...800...59V), which is affected by
systematics in the photometric data of the MOST satellite
(A. Vanderburg, private communication).
Note (2): for tw (This work): the planet radius was newly determined from the
Rp/Rs transit parameter in the literature and the stellar radius Rs as
reported in Table 1.
Note (3): equilibrium temperature by considering a null Bond albedo and full
heat redistribution from the day to the night side
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 A2 -- Ref Reference number
4- 22 A19 --- BibCode BibCode
24- 43 A20 --- Aut Author's name
45- 66 A22 --- Com Comments
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Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- System Name of the planetary system or host star
13- 16 A4 --- n_System [HN-1 HN-2] Note on System (1)
18- 28 F11.6 d Time Epochs of measurements TDB (BJD-2450000)
33- 41 F9.2 m/s RV Radial velocity (2)
46- 50 F5.2 m/s e_RV 1-sigma uncertainty of the radial velocity
55- 62 F8.2 m/s FWHM ? Full with at half maximum of the
cross correlation function
67- 71 F5.2 m/s e_FWHM ? 1-sigma uncertainty of the
full with at half maximum
76- 80 F5.2 % C ? Contrast of the cross correlation function
86- 89 F4.2 % e_C ? 1-sigma uncertainty of the contrast
94-100 F7.2 m/s BIS ? Bisector span of the
cross correlation function
105-109 F5.2 m/s e_BIS ? 1-sigma uncertainty of the bisector span
115-119 F5.3 --- SMW ? CaII H&K Mount Wilson S index (3)
125-129 F5.3 --- e_SMW ? 1-sigma uncertainty of the S index (3)
134-139 F6.3 [-] log(R'HK) ? logarithm of the R'HK activity index (3)
145-149 F5.3 [-] e_log(R'HK) ? 1-sigma uncertainty of the logarithm of the
R'HK activity index (3)
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Note (1): HN-1 and HN-2 for Kepler-10, Kepler-19, Kepler-22, and Kepler-102
indicate two HARPS-N datasets obtained before and after 6200 BJD_TDB-2450000,
respectively. They should be considered as two independent datasets because
they were acquired before and after the replacement of the HARPS-N CCD,
which gives a slightly different radial-velocity zero point for the two
datasets.
Note (2): For Kepler-10, H-2 RV are relative velocities.
Note (3): Activity indicators are not reported for K2-3 because its radial
radial velocities were extracted with a different pipeline from the
HARPS-N Data Reduction Software v2.3.5, that is the TERRA pipeline
log(R'hk) measurements are not available for K2-135/GJ9827 because the B-V
of the host star is greater than 1.2
The S index and log(R'hk) activity indicators could not be computed for a
couple of low S/N spectra, in which case they are not reported
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Acknowledgements:
Aldo Bonomo, aldo.bonomo(at)inaf.it
(End) Patricia Vannier [CDS] 22-Aug-2023